Scaling Relations for Collision-less Dark Matter Turbulence

Many scaling relations are observed for self-gravitating systems in the universe. We explore the consistent understanding of them from a simple principle based on the proposal that the collision-less dark matter fluid terns into a turbulent state, i.e. dark turbulence, after crossing the caustic surface in the non-linear stage. The dark turbulence will not eddy dominant reflecting the collision-less property. After deriving Kolmogorov scaling laws from Navier-Stokes equation by the method similar to the one for Smoluchowski coagulation equation, we apply this to several observations such as the scale-dependent velocity dispersion, mass-luminosity ratio, magnetic fields, and mass-angular momentum relation, power spectrum of density fluctuations. They all point the concordant value for the constant energy flow per mass: $0.3 cm^2/sec^3$, which may be understood as the speed of the hierarchical coalescence process in the cosmic structure formation.Comment: 26 pages, 6 figure

Toward Understanding the origin of the Fundamental Plane for Early-Type Galaxies

We present a panoramic review of several observational and theoretical aspects of the modern astrophysical research about the origin of the Fundamental Plane (FP) relation for Early-Type Galaxies (ETGs). The discussion is focused on the problem of the tilt and the tightness of the FP, and on the attempts to derive the luminosity evolution of ETGs with redshift. Finally, a number of observed features in the FP are interpreted from the standpoint of a new theoretical approach based on the two-component tensor virial theorem.Comment: 30 pages, 3 figure

A GLIMPSE into the Nature of Galactic Mid-IR Excesses

We investigate the nature of the mid-IR excess for 31 intermediate-mass stars that exhibit an 8 micron excess in either the Galactic Legacy Infrared Mid-Plane Survey Extraordinaire or the Mid-Course Space Experiment using high resolution optical spectra to identify stars surrounded by warm circumstellar dust. From these data we determine projected stellar rotational velocities and estimate stellar effective temperatures for the sample. We estimate stellar ages from these temperatures, parallactic distances, and evolutionary models. Using MIPS [24] measurements and stellar parameters we determine the nature of the infrared excess for 19 GLIMPSE stars. We find that 15 stars exhibit Halpha emission and four exhibit Halpha absorption. Assuming that the mid-IR excesses arise in circumstellar disks, we use the Halpha fluxes to model and estimate the relative contributions of dust and free-free emission. Six stars exhibit Halpha fluxes that imply free-free emission can plausibly explain the infrared excess at [24]. These stars are candidate classical Be stars. Nine stars exhibit Halpha emission, but their Halpha fluxes are insufficient to explain the infrared excesses at [24], suggesting the presence of a circumstellar dust component. After the removal of the free-free component in these sources, we determine probable disk dust temperatures of Tdisk~300-800 K and fractional infrared luminosities of L(IR)/L(*)~10^-3. These nine stars may be pre-main-sequence stars with transitional disks undergoing disk clearing. Three of the four sources showing Halpha absorption exhibit circumstellar disk temperatures ~300-400 K, L(IR)/L(*)~10^-3, IR colors K-[24]< 3.3, and are warm debris disk candidates. One of the four Halpha absorption sources has K-[24]> 3.3 implying an optically thick outer disk and is a transition disk candidate.Comment: 17 figures. Accepted for publication in Ap

Cosmology, Oscillating Physics and Oscilllating Biology

According to recent reports there is an excess correlation and an apparent regularity in the galaxy one-dimensional polar distribution with a characteristic scale of 128 $h^{-1}$ Mpc. This aparent spatial periodicity can be naturally explained by a time oscillation of the gravitational constant $G$. On the other hand, periodic growth features of bivalve and coral fossiles appear to show a periodic component in the time dependence of the number of days per year. In this letter we show that a time oscillating gravitational constant with similar period and amplitude can explain such a feature.Comment: 9 pages. latex using revtex. This revised version is supposed to be free of e-mail nois

Astrometry and geodesy with radio interferometry: experiments, models, results

Summarizes current status of radio interferometry at radio frequencies between Earth-based receivers, for astrometric and geodetic applications. Emphasizes theoretical models of VLBI observables that are required to extract results at the present accuracy levels of 1 cm and 1 nanoradian. Highlights the achievements of VLBI during the past two decades in reference frames, Earth orientation, atmospheric effects on microwave propagation, and relativity.Comment: 83 pages, 19 Postscript figures. To be published in Rev. Mod. Phys., Vol. 70, Oct. 199

Rotation Curve of Galaxies by the Force Induced by Mass of Moving Particles

We suggest that there is a novel force which is generated by the mass of relatively moving particles. The new force which we named Mirinae Force is a counterpart of the magnetic force operating between electrically charged moving particles. Instead of using the conventional dark matter, we applied the mirinae force to a particular model system of the spiral galaxy in which most of the galaxy's mass is located within the central region where some portion of the inner mass is in revolving motion at a relativistic speed. The calculation yielded three important results that illustrate the existence of mirinae force and validate the proposed model: First, the mirinae force in this model explains why most of the matters in the galactic disk are in the circular motion which is similar to cycloid. Second, the mirinae force well explains not only the flat rotation curve but also the varied slope of the rotation curve observed in the spiral galaxies. Third, at the flat velocity of 220 Km/s, the inner mass of the Milky Way calculated by using the proposed model is 6.0\times10^11 M\odot, which is very close to 5.5\times10^11 M\odot (r <50 Kpc, including Leo I) estimated by using the latest kinematic information. This means that the mirinae force well takes the place of the dark matter of the Milky Way

Global and Local Three-dimensional Studies of The Residual Vector Field from 2MASS and Hipparcos-2 Catalog

[EN] The Gaia mission will provide a six-parameter solution for millions of stars, including a tridimensional map of our Galaxy. The estimation of distances has been made for the Tycho-Gaia Astrometric Solution (TGAS), while to contrast the proper motions it is interesting to consider positions from the different Gaia Data Release with older ones given in ground-based massive catalogs. This process has been followed to build, for example, the PMA catalog using the 2MASS. Our aim is to improve the positions of this catalog (although the process is applicable to any other). The first stage, presented here, consists of carrying out a three-dimensional study using vector spherical harmonics (VSH) development of the systematisms in position for the stars common with Hipparcos-2; we take into account the distances, magnitudes, and spectral types. To this aim, we use linear polynomial regression of first order that fits vector fields and the derivatives of their components. We verify that the coefficients of the developments of first order have different behavior according to the characteristics of stars and distances. To deepen the study, we focus on the conservative component of the field, applying the Helmholtz theorem. Each potential function is obtained solving a Poisson equation on the sphere, after finding the divergence of the corresponding vector field. Both vector and potential fields present patterns, at certain points, that depend on the three considered parameters (distance, magnitude, and spectral type); their sources and shrinks correspond to maxima and minima. In this sense, we observe that these critical points are also critical points of the surface that represents the VT magnitude of Tycho-2, which makes sense because this catalog was used in the reduction of 2MASS positions. Finally, we selected some stars near the critical points of the vector fields and apply the adjustments obtained in the previous sections. The difference with the positions in DR1 allows us to compare the proper motions: those from the PMA and those induced after our corrections.This paper was partially supported by the UJI-B2016-18, 16I356 project.Marco Castillo, FJ.; Martínez Uso, MJ.; Lopez, J. (2019). Global and Local Three-dimensional Studies of The Residual Vector Field from 2MASS and Hipparcos-2 Catalog. Publications of the Astronomical Society of the Pacific. 131(998):1-22. https://doi.org/10.1088/1538-3873/aaed5dS122131998Akhmetov, V. S., Fedorov, P. N., Velichko, A. B., & Shulga, V. M. (2017). The PMA Catalogue: 420 million positions and absolute proper motions. Monthly Notices of the Royal Astronomical Society, 469(1), 763-773. doi:10.1093/mnras/stx812Arenou, F., Luri, X., Babusiaux, C., Fabricius, C., Helmi, A., Robin, A. C., … Bragaglia, A. (2017). Gaia Data Release 1. Astronomy & Astrophysics, 599, A50. doi:10.1051/0004-6361/201629895Astraatmadja, T. L., & Bailer-Jones, C. A. L. (2016). ESTIMATING DISTANCES FROM PARALLAXES. II. PERFORMANCE OF BAYESIAN DISTANCE ESTIMATORS ON AGAIA-LIKE CATALOGUE. The Astrophysical Journal, 832(2), 137. doi:10.3847/0004-637x/832/2/137Astraatmadja, T. L., & Bailer-Jones, C. A. L. (2016). ESTIMATING DISTANCES FROM PARALLAXES. III. DISTANCES OF TWO MILLION STARS IN THEGaiaDR1 CATALOGUE. The Astrophysical Journal, 833(1), 119. doi:10.3847/1538-4357/833/1/119Bailer-Jones, C. A. L. (2015). Estimating Distances from Parallaxes. Publications of the Astronomical Society of the Pacific, 127(956), 994-1009. doi:10.1086/683116Davies, G. R., Lund, M. N., Miglio, A., Elsworth, Y., Kuszlewicz, J. S., North, T. S. H., … Schofield, M. (2017). Using red clump stars to correct theGaiaDR1 parallaxes. Astronomy & Astrophysics, 598, L4. doi:10.1051/0004-6361/201630066Gontcharov, G. A. (2017). Systematic error of the Gaia DR1 TGAS parallaxes from data for the red giant clump. Astronomy Letters, 43(8), 545-558. doi:10.1134/s1063773717060044Jeffreys, S. H. (1967). A Completeness Theorem for Expansions of a Vector Function in Spherical Harmonics. Geophysical Journal International, 12(5), 465-468. doi:10.1111/j.1365-246x.1967.tb03126.xLindegren, L., Lammers, U., Bastian, U., Hernández, J., Klioner, S., Hobbs, D., … Butkevich, A. (2016). GaiaData Release 1. Astronomy & Astrophysics, 595, A4. doi:10.1051/0004-6361/201628714Lindegren, L., Lammers, U., Hobbs, D., O’Mullane, W., Bastian, U., & Hernández, J. (2012). The astrometric core solution for theGaiamission. Astronomy & Astrophysics, 538, A78. doi:10.1051/0004-6361/201117905Makarov, V. V., & Murphy, D. W. (2007). The Local Stellar Velocity Field via Vector Spherical Harmonics. The Astronomical Journal, 134(1), 367-375. doi:10.1086/518242Marco, F. J., Martínez, M. J., & López, J. A. (2004). A critical discussion on parametric and nonparametric regression methods applied to Hipparcos-FK5 residuals. Astronomy & Astrophysics, 418(3), 1159-1170. doi:10.1051/0004-6361:20034441Marco, F. J., Martínez, M. J., & López, J. A. (2013). Homogenization in compiling ICRF combined catalogs. Astronomy & Astrophysics, 558, A98. doi:10.1051/0004-6361/201321995Marco, F. J., Martínez, M. J., & López, J. A. (2015). APPLICATION OF VECTOR SPHERICAL HARMONICS AND KERNEL REGRESSION TO THE COMPUTATIONS OF OMM PARAMETERS. The Astronomical Journal, 149(4), 129. doi:10.1088/0004-6256/149/4/129Masry, E., & Jianqing Fan. (1997). Local Polynomial Estimation of Regression Functions for Mixing Processes. Scandinavian Journal of Statistics, 24(2), 165-179. doi:10.1111/1467-9469.00056Michalik, D., Lindegren, L., & Hobbs, D. (2015). TheTycho-Gaiaastrometric solution. Astronomy & Astrophysics, 574, A115. doi:10.1051/0004-6361/201425310Michalik, D., Lindegren, L., Hobbs, D., & Lammers, U. (2014). Joint astrometric solution of HIPPARCOS andGaia. Astronomy & Astrophysics, 571, A85. doi:10.1051/0004-6361/201424606Mignard, F., & Klioner, S. (2012). Analysis of astrometric catalogues with vector spherical harmonics. Astronomy & Astrophysics, 547, A59. doi:10.1051/0004-6361/201219927De Ridder, J., Molenberghs, G., Eyer, L., & Aerts, C. (2016). Asteroseismic versusGaiadistances: A first comparison. Astronomy & Astrophysics, 595, L3. doi:10.1051/0004-6361/201629799Roeser, S., Demleitner, M., & Schilbach, E. (2010). THE PPMXL CATALOG OF POSITIONS AND PROPER MOTIONS ON THE ICRS. COMBINING USNO-B1.0 AND THE TWO MICRON ALL SKY SURVEY (2MASS). The Astronomical Journal, 139(6), 2440-2447. doi:10.1088/0004-6256/139/6/2440Röser, S., Schilbach, E., Schwan, H., Kharchenko, N. V., Piskunov, A. E., & Scholz, R.-D. (2008). PPM-Extended (PPMX) – a catalogue of positions and proper motions. Astronomy & Astrophysics, 488(1), 401-408. doi:10.1051/0004-6361:200809775Schönrich, R., & Aumer, M. (2017). Assessing distances and consistency of kinematics in Gaia/TGAS. Monthly Notices of the Royal Astronomical Society, 472(4), 3979-3998. doi:10.1093/mnras/stx2189Schwan, H. (2001). An analytical representation of the systematic differences HIPPARCOS-FK5. Astronomy & Astrophysics, 367(3), 1078-1086. doi:10.1051/0004-6361:20000521Simonoff, J. S. (1996). Smoothing Methods in Statistics. Springer Series in Statistics. doi:10.1007/978-1-4612-4026-6Skrutskie, M. F., Cutri, R. M., Stiening, R., Weinberg, M. D., Schneider, S., Carpenter, J. M., … Wheelock, S. (2006). The Two Micron All Sky Survey (2MASS). The Astronomical Journal, 131(2), 1163-1183. doi:10.1086/498708Stassun, K. G., & Torres, G. (2016). EVIDENCE FOR A SYSTEMATIC OFFSET OF −0.25 mas IN THE GAIA DR1 PARALLAXES. The Astrophysical Journal, 831(1), L6. doi:10.3847/2041-8205/831/1/l6Van Leeuwen, F. (2007). Validation of the new Hipparcos reduction. Astronomy & Astrophysics, 474(2), 653-664. doi:10.1051/0004-6361:20078357Van Leeuwen, F. (Ed.). (2007). Hipparcos, the New Reduction of the Raw Data. Astrophysics and Space Science Library. doi:10.1007/978-1-4020-6342-8Vityazev, V. V., & Tsvetkov, A. S. (2009). Analysis of the three-dimensional stellar velocity field using vector spherical functions. Astronomy Letters, 35(2), 100-113. doi:10.1134/s1063773709020042Vityazev, V. V., & Tsvetkov, A. S. (2011). Application of vector spherical harmonics for kinematic analysis of stars from zonal catalogues. Astronomy Letters, 37(12), 874-887. doi:10.1134/s1063773711120103Vityazev, V. V., & Tsvetkov, A. S. (2013). UCAC4: Stellar kinematics with vector spherical functions. Astronomische Nachrichten, 334(8), 760-768. doi:10.1002/asna.201311917Vityazev, V. V., & Tsvetkov, A. S. (2014). Intercomparison of kinematics derived from catalogues UCAC4, PPMXL and XPM with vector spherical harmonics. Monthly Notices of the Royal Astronomical Society, 442(2), 1249-1264. doi:10.1093/mnras/stu953Vityazev, V. V., & Tsvetkov, A. S. (2015). Systematic differences between the positions and proper motions of stars from the PPMXL and UCAC4 catalogs. Astronomy Letters, 41(7), 317-333. doi:10.1134/s1063773715070063Vityazev, V. V., Tsvetkov, A. S., Petrov, S. D., Trofimov, D. A., & Kiyaev, V. I. (2017). Properties of the Tycho-2 catalogue from Gaia data release. Astronomy Letters, 43(11), 730-750. doi:10.1134/s106377371711007xVityazev, V. V., Tsvetkov, A. S., Bobylev, V. V., & Bajkova, A. T. (2017). Galactic Kinematics Derived From Data in the RAVE5, UCAC4, PPMXL, and Gaia TGAS Catalogs. Astrophysics, 60(4), 462-483. doi:10.1007/s10511-017-9499-0Vityazev, V. V., Tsvetkov, A. S., Petrov, S. D., & Trofimov, D. A. (2017). Comparison of XPM and UCAC4 catalogues in the galactic coordinate system. Astronomische Nachrichten, 338(4), 489-502. doi:10.1002/asna.201613220Zacharias, N., Finch, C., & Frouard, J. (2017). UCAC5: New Proper Motions UsingGaiaDR1. 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Rotation of the Universe and the angular momenta of celestial bodies

We discuss the equation of motion of the rotating homogenous and isotropic model of the Universe. We show that the model predicts the presence of a minimum in the relation between the mass of an astronomical object and its angular momentum. We show that this relation appears to be universal, and we predict the masses of structures with minimal angular momenta in agreement with observations. In such a manner we suggest the possibility at acquirement of angular momenta of celestial bodies during their formation from the global rotation of the Universe.Comment: 10 pages 2 figure

Genome sequencing and population genomic analyses provide insights into the adaptive landscape of silver birch

201